過去數十年的天文觀測，揭示了恆星主要形成於帶有磁場和紊流的分子雲中。然而，磁場如何影響恆星形成的過程仍然並未被了解。恆星形成理論認為磁場有助於平衡分子雲內的重力、降低恆星形成的速率、並能協助年輕恆星移除角動量。儘管如此，由於觀測上的困難，這些理論上的預測很少能被觀測驗證。IC5146分子雲是一個知名的恆星形成區域，擁有著處於各種不同演化階段的原恆星。過去數年赫歇爾(Herschel)太空望遠鏡發現，IC5146分子雲主要由細緻的絲狀結構所組成，而年輕恆星的空間分部符合這些絲狀結構，顯示了恆星應該是從這些絲狀結構中形成的，而且恆星形成很可能是由大尺度的紊流所觸發。然而，這些分析缺少了磁場的資訊，而磁場又可能是影響恆星形成的重要因素。因此，本篇論文的主要目標即為探討磁場在這樣一個充滿紊流的恆星形成區中，在恆星形成的程序中，扮演著怎麼樣的角色。我們在過去數年進行了可見光、紅外線、次毫米波的偏極化觀測，藉由觀測塵埃輻射的偏極方向來描繪磁場的結構。有了這些觀測資料，我們首先分析了分子雲中的偏極效率和雲氣密度的關係，證實我們的偏極化觀測真的能追溯分子雲內部的磁場。其次，我們發現觀測數據描繪出的磁場結構相當均勻，不符合紊流主宰的模型預測，而我們估算出的大尺度磁場強度也足以支撐分子雲的重力。直到次秒差距尺度，在最緻密的絲狀結構與原恆星核中，重力的強度才逐漸能克服磁場，以此觸發恆星的形成。以上我們的發現，大部分都支持假定強磁場的恆星演化模型，這些模型預期大尺度的磁場能夠支撐大尺度的分子雲結構，而在緻密區域磁場會逐漸消散，因而重力能進一步主導以產生恆星。

Observations over the last few decades have revealed that stars predominately form within magnetized and turbulent filamentary clouds. How magnetic fields regulate star formation, however, is still poorly understood. Theoretical works have suggested that magnetic fields could be important in supporting molecular clouds, suppressing the star formation rate, and removing angular momentum. Nonetheless, measurements of magnetic field morphologies and strength are still too rare to test these theories. The IC5146 cloud is a well-known star-forming region with young stellar objects in a variety of evolutionary stage. Recent Herschel telescope has revealed that the IC5146 cloud is composed of a filamentary cloud, and the spatial distribution of young stars is consistent with these filaments. This suggests that the filaments are the birth sites of young stars, possibly triggered by the large scale MHD turbulence. However, these analysis lacks of the information of magnetic fields, and it would be critical to understand what the role of magnetic fields is in the turbulent star-forming region. The main goal of this thesis is to investigate the role of the magnetic fields while the filamentary clouds (pc scales) evolve to cores (sub-parsec scales). We performed optical, near-infrared, and sub-millimeter polarization observations to probe the magnetic fields over the IC5146 cloud from few pc to 0.1 pc scale. With these observed data, we analyzed how polarization efficiency varies with the density, and show that our polarization data can really trace the magnetic field within the cloud. In addition, we found that the pc scale magnetic field is almost uniform, and the magnetic fields is sufficiently strong to support the gravity. However, the gravity gradually overcomes the support of magnetic field within the dense filaments and cores at sub-parsec scale. These features favor the strong magnetic field star formation theory, which expects a magnetic field important in supporting and regulating the star formation until magnetic fields are dissipated.

Contents
摘要 1
Abstract 2
List of Figures 6
List of Tables 9
Chapter 1. Introduction: B-fields in Molecular Clouds 10
1.1. Theoretical Background 10
1.1.1 Strong B-field Model 10
1.1.2 Weak B-field Model 10
1.2 Observational Results 11
2. Multiwavelength Polarimetry of the Filamentary Cloud IC5146 I. Dust Properties 13
2.1. Introduction 13
2.2 Observations and Data Reduction 16
2.2.1 AIMPOL Polarimetry 17
2.2.2 TRIPOL Polarimetry 18
2.2.3 Mimir Polarimetry 18
2.3 Results 19
2.3.1 The Polarization Catalog 19
2.3.2 Consistency in P.A. between Multiple Wavelengths 22
2.3.3 Negligible Foreground Contamination 23
2.4 Analysis 24
2.4.1 NICER Extinction 24
2.4.2 Polarization Efficiency 26
2.4.3 Wavelength Dependence of Polarization using the Serkowski Relation 31
2.4.4 “Polarization Color” as a Constraint on λmax 32
2.5 Discussion 38
2.5.1 Evolution of Dust Grains 38
2.5.2 How Deep Into a Cloud Can Polarization Be Used to Reveal B fields? 39
2.5.3 The Diverse PE in Low-AV Regions 40
2.5.4 The Breakpoint in PE–AV Relations 41
2.6 Conclusions 42
3. Multiwavelength Polarimetry of the Filamentary Cloud IC5146 II. Magnetic Field Structures 44
3.1. Introduction 44
3.2 Analysis 47
3.2.1 The Distance to the IC5146 system 47
3.2.2 Magnetic Field Morphology 50
3.2.3 Magnetic Field Strength over the IC5146 Cloud 55
3.2.4 Magnetic Strength versus Density 63
3.2.5. Mass-to-Magnetic Flux ratio 73
3.3 Discussion 76
3.3.1 Magnetic Field Morphology 76
3.3.2 Magnetic Field Strength 77
3.3.3 B-n Relation 77
3.4 Conclusions 79
Chapter 4. JCMT BISTRO Survey: Magnetic Fields within The Hub-Filament Structure in IC 5146 80
4.1. Introduction 80
4.2. OBSERVATIONS 83
4.2.1 Data Acquisition and Reduction Techniques 83
4.2.1 CO contamination 86
4.3 Results and Analysis 86
4.3.1 Magnetic Field Morphology 86
4.3.2 Polarization Efficiency 92
4.3.3 Polarization Efficiency–AV Dependence 94
4.3.4 Orientation of Clumps and Magnetic Fields 98
4.3.5 Magnetic Field Strength in IC5146 101
4.3.6 Gravitational Stability of Clumps 107
4.4 Discussion 108
4.4.1 The Origin of the Core-Scale HFS 108
4.4.2 The Alignment between Local Magnetic Fields and Clumps 111
4.5 Conclusions 112
4.6 Appendix: Bias on Determination of P vs. I relation 113
Chapter 5. Conclusions 116
Reference 119

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